DIFFERENTIAL ROTATION IN STELLAR CONVECTIVE ENVELOPES

The model for solar global circulation is used to calculate the differ ential rotation in stellar convective envelopes. The nonuniformity of angular velocity within the convection zone increases with rotation pe riod and with stellar mass. For young stars that arrive at the main se quence, the model predicts a magnitude of the differential rotation of no more than 1%. As the rotation slows down with stellar age, this ma gnitude reaches greater than or similar to 10%. For main-sequence star s, we failed to find an example of simultaneously rapid and highly non uniform rotation. This combination, however, can take place in giant s tars of luminosity class III. Possible implications of the predictions of the model for stellar dynamo are discussed.